المؤلفون: Nielsen, Eric L, De Rosa, Robert J, Macintosh, Bruce, Wang, Jason J, Ruffio, Jean-Baptiste, Chiang, Eugene, Marley, Mark S, Saumon, Didier, Savransky, Dmitry, Ammons, S Mark, Bailey, Vanessa P, Barman, Travis, Blain, Célia, Bulger, Joanna, Burrows, Adam, Chilcote, Jeffrey, Cotten, Tara, Czekala, Ian, Doyon, Rene, Duchêne, Gaspard, Esposito, Thomas M, Fabrycky, Daniel, Fitzgerald, Michael P, Follette, Katherine B, Fortney, Jonathan J, Gerard, Benjamin L, Goodsell, Stephen J, Graham, James R, Greenbaum, Alexandra Z, Hibon, Pascale, Hinkley, Sasha, Hirsch, Lea A, Hom, Justin, Hung, Li-Wei, Dawson, Rebekah Ilene, Ingraham, Patrick, Kalas, Paul, Konopacky, Quinn, Larkin, James E, Lee, Eve J, Lin, Jonathan W, Maire, Jérôme, Marchis, Franck, Marois, Christian, Metchev, Stanimir, Millar-Blanchaer, Maxwell A, Morzinski, Katie M, Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Perrin, Marshall, Poyneer, Lisa, Pueyo, Laurent, Rafikov, Roman R, Rajan, Abhijith, Rameau, Julien, Rantakyrö, Fredrik T, Ren, Bin, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Tallis, Melisa, Thomas, Sandrine, Ward-Duong, Kimberly, Wolff, Schuyler

المصدر: The Astronomical Journal. 158(1)

مصطلحات موضوعية: instrumentation: adaptive optics, planetary systems, planets and satellites: detection, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics

الوصف: We present a statistical analysis of the first 300 stars observed by the Gemini Planet Imager Exoplanet Survey. This subsample includes six detected planets and three brown dwarfs; from these detections and our contrast curves we infer the underlying distributions of substellar companions with respect to their mass, semimajor axis, and host stellar mass. We uncover a strong correlation between planet occurrence rate and host star mass, with stars M ∗ >1.5 M o more likely to host planets with masses between 2 and 13M Jup and semimajor axes of 3-100 au at 99.92% confidence. We fit a double power-law model in planet mass (m) and semimajor axis (a) for planet populations around high-mass stars (M ∗ >1.5 M o) of the form , finding α = -2.4 +0.8 and β = -2.0 +0.5, and an integrated occurrence rate of % between 5-13M Jup and 10-100 au. A significantly lower occurrence rate is obtained for brown dwarfs around all stars, with % of stars hosting a brown dwarf companion between 13-80M Jup and 10-100 au. Brown dwarfs also appear to be distributed differently in mass and semimajor axis compared to giant planets; whereas giant planets follow a bottom-heavy mass distribution and favor smaller semimajor axes, brown dwarfs exhibit just the opposite behaviors. Comparing to studies of short-period giant planets from the radial velocity method, our results are consistent with a peak in occurrence of giant planets between ∼1 and 10 au. We discuss how these trends, including the preference of giant planets for high-mass host stars, point to formation of giant planets by core/pebble accretion, and formation of brown dwarfs by gravitational instability.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/06w3x56nTest

المؤلفون: Esposito, Thomas M, Duchêne, Gaspard, Kalas, Paul, Rice, Malena, Choquet, Élodie, Ren, Bin, Perrin, Marshall D, Chen, Christine H, Arriaga, Pauline, Chiang, Eugene, Nielsen, Eric L, Graham, James R, Wang, Jason J, De Rosa, Robert J, Follette, Katherine B, Ammons, S Mark, Ansdell, Megan, Bailey, Vanessa P, Barman, Travis, Bruzzone, Juan Sebastián, Bulger, Joanna, Chilcote, Jeffrey, Cotten, Tara, Doyon, Rene, Fitzgerald, Michael P, Goodsell, Stephen J, Greenbaum, Alexandra Z, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Konopacky, Quinn, Larkin, James E, Macintosh, Bruce, Maire, Jérôme, Marchis, Franck, Marois, Christian, Mazoyer, Johan, Metchev, Stanimir, Millar-Blanchaer, Maxwell A, Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Poyneer, Lisa, Pueyo, Laurent, Rajan, Abhijith, Rameau, Julien, Rantakyrö, Fredrik T, Ryan, Dominic, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Rémi, Thomas, Sandrine, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane, Wolff, Schuyler

المصدر: The Astronomical Journal. 156(2)

مصطلحات موضوعية: circumstellar matter, infrared: planetary systems, stars: individual, techniques: high angular resolution, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics

الوصف: We present new high resolution imaging of a light-scattering dust ring and halo around the young star HD 35841. Using spectroscopic and polarimetric data from the Gemini Planet Imager in H-band (1.6 μm), we detect the highly inclined (i = 85°) ring of debris down to a projected separation of ∼12 au (∼0.″12) for the first time. Optical imaging from HST/STIS shows a smooth dust halo extending outward from the ring to >140 au (>1.″4). We measure the ring's scattering phase function and polarization fraction over scattering angles of 22°-125°, showing a preference for forward scattering and a polarization fraction that peaks at ∼30% near the ansae. Modeling of the scattered-light disk indicates that the ring spans radii of ∼60-220 au, has a vertical thickness similar to that of other resolved dust rings, and contains grains as small as 1.5 μm in diameter. These models also suggest the grains have a low porosity, are more likely to consist of carbon than astrosilicates, and contain significant water ice. The halo has a surface brightness profile consistent with that expected from grains pushed by radiation pressure from the main ring onto highly eccentric but still bound orbits. We also briefly investigate arrangements of a possible inner disk component implied by our spectral energy distribution models, and speculate about the limitations of Mie theory for doing detailed analyses of debris disk dust populations.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/7bp5r7bnTest

المؤلفون: Greenbaum, Alexandra Z, Pueyo, Laurent, Ruffio, Jean-Baptiste, Wang, Jason J, De Rosa, Robert J, Aguilar, Jonathan, Rameau, Julien, Barman, Travis, Marois, Christian, Marley, Mark S, Konopacky, Quinn, Rajan, Abhijith, Macintosh, Bruce, Ansdell, Megan, Arriaga, Pauline, Bailey, Vanessa P, Bulger, Joanna, Burrows, Adam S, Chilcote, Jeffrey, Cotten, Tara, Doyon, Rene, Duchêne, Gaspard, Fitzgerald, Michael P, Follette, Katherine B, Gerard, Benjamin, Goodsell, Stephen J, Graham, James R, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Kalas, Paul, Larkin, James E, Maire, Jérôme, Marchis, Franck, Metchev, Stanimir, Millar-Blanchaer, Maxwell A, Nielsen, Eric L, Norton, Andrew, Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Perrin, Marshall D, Poyneer, Lisa, Rantakyrö, Fredrik T, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Rémi, Thomas, Sandrine, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane, Wolff, Schuyler

المصدر: The Astronomical Journal. 155(6)

مصطلحات موضوعية: planets and satellites: gaseous planets, stars: individual, Astronomical and Space Sciences, Astronomy & Astrophysics

الوصف: We explore KLIP forward modeling spectral extraction on Gemini Planet Imager coronagraphic data of HR 8799, using PyKLIP, and show algorithm stability with varying KLIP parameters. We report new and re-reduced spectrophotometry of HR 8799 c, d, and e in the H and K bands. We discuss a strategy for choosing optimal KLIP PSF subtraction parameters by injecting simulated sources and recovering them over a range of parameters. The K1/K2 spectra for HR 8799 c and d are similar to previously published results from the same data set. We also present a K-band spectrum of HR 8799 e for the first time and show that our H-band spectra agree well with previously published spectra from the VLT/SPHERE instrument. We show that HR 8799 c and d show significant differences in their H and K spectra, but do not find any conclusive differences between d and e, nor between c and e, likely due to large error bars in the recovered spectrum of e. Compared to M-, L-, and T-type field brown dwarfs, all three planets are most consistent with mid- and late-L spectral types. All objects are consistent with low gravity, but a lack of standard spectra for low gravity limit the ability to fit the best spectral type. We discuss how dedicated modeling efforts can better fit HR 8799 planets' near-IR flux, as well as how differences between the properties of these planets can be further explored.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/0k83q01rTest

المؤلفون: Wang, Jason J, Perrin, Marshall D, Savransky, Dmitry, Arriaga, Pauline, Chilcote, Jeffrey K, De Rosa, Robert J, Millar-Blanchaer, Maxwell A, Marois, Christian, Rameau, Julien, Wolff, Schuyler G, Shapiro, Jacob, Ruffio, Jean-Baptiste, Maire, Jérôme, Marchis, Franck, Graham, James R, Macintosh, Bruce, Ammons, S Mark, Bailey, Vanessa P, Barman, Travis S, Bruzzone, Sebastian, Bulger, Joanna, Cotten, Tara, Doyon, René, Duchêne, Gaspard, Fitzgerald, Michael P, Follette, Katherine B, Goodsell, Stephen, Greenbaum, Alexandra Z, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Kalas, Paul, Konopacky, Quinn M, Larkin, James E, Marley, Mark S, Metchev, Stanimir, Nielsen, Eric L, Oppenheimer, Rebecca, Palmer, David W, Patience, Jennifer, Poyneer, Lisa A, Pueyo, Laurent, Rajan, Abhijith, Rantakyrö, Fredrik T, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Thomas, Sandrine, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane J

المصدر: Journal of Astronomical Telescopes Instruments and Systems. 4(1)

مصطلحات موضوعية: high contrast imaging, exoplanets, circumstellar disks, data processing, Gemini planet imager, Data Cruncher, astro-ph.IM, astro-ph.EP, Mathematical Sciences, Physical Sciences

الوصف: The Gemini Planet Imager Exoplanet Survey (GPIES) is a multiyear direct imaging survey of 600 stars to discover and characterize young Jovian exoplanets and their environments. We have developed an automated data architecture to process and index all data related to the survey uniformly. An automated and flexible data processing framework, which we term the Data Cruncher, combines multiple data reduction pipelines (DRPs) together to process all spectroscopic, polarimetric, and calibration data taken with GPIES. With no human intervention, fully reduced and calibrated data products are available less than an hour after the data are taken to expedite follow up on potential objects of interest. The Data Cruncher can run on a supercomputer to reprocess all GPIES data in a single day as improvements are made to our DRPs. A backend MySQL database indexes all files, which are synced to the cloud, and a front-end web server allows for easy browsing of all files associated with GPIES. To help observers, quicklook displays show reduced data as they are processed in real time, and chatbots on Slack post observing information as well as reduced data products. Together, the GPIES automated data processing architecture reduces our workload, provides real-Time data reduction, optimizes our observing strategy, and maintains a homogeneously reduced dataset to study planet occurrence and instrument performance.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/26g8z8wnTest

المؤلفون: Nielsen, Eric L, De Rosa, Robert J, Rameau, Julien, Wang, Jason J, Esposito, Thomas M, Millar-Blanchaer, Maxwell A, Marois, Christian, Vigan, Arthur, Ammons, S Mark, Artigau, Etienne, Bailey, Vanessa P, Blunt, Sarah, Bulger, Joanna, Chilcote, Jeffrey, Cotten, Tara, Doyon, René, Duchêne, Gaspard, Fabrycky, Daniel, Fitzgerald, Michael P, Follette, Katherine B, Gerard, Benjamin L, Goodsell, Stephen J, Graham, James R, Greenbaum, Alexandra Z, Hibon, Pascale, Hinkley, Sasha, Hung, Li-Wei, Ingraham, Patrick, Jensen-Clem, Rebecca, Kalas, Paul, Konopacky, Quinn, Larkin, James E, Macintosh, Bruce, Maire, Jérôme, Marchis, Franck, Metchev, Stanimir, Morzinski, Katie M, Murray-Clay, Ruth A, Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Perrin, Marshall, Poyneer, Lisa, Pueyo, Laurent, Rafikov, Roman R, Rajan, Abhijith, Rantakyrö, Fredrik T, Ruffio, Jean-Baptiste, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Thomas, Sandrine, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane, Wolff, Schuyler

المصدر: The Astronomical Journal. 154(6)

مصطلحات موضوعية: astrometry, instrumentation: adaptive optics, planets and satellites: detection, stars: individual, techniques: image processing, techniques: spectroscopic, astro-ph.EP, astro-ph.SR, Astronomical and Space Sciences, Astronomy & Astrophysics

الوصف: We present evidence that the recently discovered, directly imaged planet HD 131399 Ab is a background star with nonzero proper motion. From new JHK1L′ photometry and spectroscopy obtained with the Gemini Planet Imager, VLT/SPHERE, and Keck/NIRC2, and a reanalysis of the discovery data obtained with VLT/SPHERE, we derive colors, spectra, and astrometry for HD 131399 Ab. The broader wavelength coverage and higher data quality allow us to reinvestigate its status. Its near-infrared spectral energy distribution excludes spectral types later than L0 and is consistent with a K or M dwarf, which are the most likely candidates for a background object in this direction at the apparent magnitude observed. If it were a physically associated object, the projected velocity of HD 131399 Ab would exceed escape velocity given the mass and distance to HD 131399 A. We show that HD 131399 Ab is also not following the expected track for a stationary background star at infinite distance. Solving for the proper motion and parallax required to explain the relative motion of HD 131399 Ab, we find a proper motion of 12.3 mas yr-1. When compared to predicted background objects drawn from a galactic model, we find this proper motion to be high but consistent with the top 4% fastest-moving background stars. From our analysis, we conclude that HD 131399 Ab is a background K or M dwarf.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/0fq714g1Test

المؤلفون: Rajan, Abhijith, Rameau, Julien, De Rosa, Robert J, Marley, Mark S, Graham, James R, Macintosh, Bruce, Marois, Christian, Morley, Caroline, Patience, Jennifer, Pueyo, Laurent, Saumon, Didier, Ward-Duong, Kimberly, Ammons, S Mark, Arriaga, Pauline, Bailey, Vanessa P, Barman, Travis, Bulger, Joanna, Burrows, Adam S, Chilcote, Jeffrey, Cotten, Tara, Czekala, Ian, Doyon, Rene, Duchêne, Gaspard, Esposito, Thomas M, Fitzgerald, Michael P, Follette, Katherine B, Fortney, Jonathan J, Goodsell, Stephen J, Greenbaum, Alexandra Z, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Johnson-Groh, Mara, Kalas, Paul, Konopacky, Quinn, Lafrenière, David, Larkin, James E, Maire, Jérôme, Marchis, Franck, Metchev, Stanimir, Millar-Blanchaer, Maxwell A, Morzinski, Katie M, Nielsen, Eric L, Oppenheimer, Rebecca, Palmer, David, Patel, Rahul I, Perrin, Marshall, Poyneer, Lisa, Rantakyrö, Fredrik T, Ruffio, Jean-Baptiste, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Rémi, Thomas, Sandrine, Vasisht, Gautam, Wallace, J Kent, Wang, Jason J, Wiktorowicz, Sloane, Wolff, Schuyler

المصدر: The Astronomical Journal. 154(1)

مصطلحات موضوعية: instrumentation: adaptive optics, planets and satellites: atmospheres, planets and satellites: composition, planets and satellites: gaseous planets, stars: individual, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics

الوصف: We present spectrophotometry spanning 1-5 μm of 51 Eridani b, a 2-10 planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new K1 (1.90-2.19 μm) and K2 (2.10-2.40 μm) spectra taken with the Gemini Planet Imager as well as an updated L P (3.76 μm) and new M S (4.67 μm) photometry from the NIRC2 Narrow camera. The new data were combined with J (1.13-1.35 μm) and H (1.50-1.80 μm) spectra from the discovery epoch with the goal of better characterizing the planet properties. The 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4 and T8), and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud-free, and patchy/intermediate-opacity clouds. The model fits suggest that 51 Eri b has an effective temperature ranging between 605 and 737 K, a solar metallicity, and a surface gravity of log(g) = 3.5-4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the spectral energy distribution (SED). From the model atmospheres, we infer a luminosity for the planet of -5.83 to -5.93 (logL/L⊙), leaving 51 Eri b in the unique position of being one of the only directly imaged planets consistent with having formed via a cold-start scenario. Comparisons of the planet SED against warm-start models indicate that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M⊕.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/9980x7sjTest

المؤلفون: Ruffio, Jean-Baptiste, Macintosh, Bruce, Wang, Jason J, Pueyo, Laurent, Nielsen, Eric L, De Rosa, Robert J, Czekala, Ian, Marley, Mark S, Arriaga, Pauline, Bailey, Vanessa P, Barman, Travis, Bulger, Joanna, Chilcote, Jeffrey, Cotten, Tara, Doyon, Rene, Duchêne, Gaspard, Fitzgerald, Michael P, Follette, Katherine B, Gerard, Benjamin L, Goodsell, Stephen J, Graham, James R, Greenbaum, Alexandra Z, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Kalas, Paul, Konopacky, Quinn, Larkin, James E, Maire, Jérôme, Marchis, Franck, Marois, Christian, Metchev, Stanimir, Millar-Blanchaer, Maxwell A, Morzinski, Katie M, Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Perrin, Marshall, Poyneer, Lisa, Rajan, Abhijith, Rameau, Julien, Rantakyrö, Fredrik T, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Thomas, Sandrine, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane, Wolff, Schuyler

المصدر: The Astrophysical Journal. 842(1)

مصطلحات موضوعية: instrumentation: adaptive optics, methods: statistical, planetary systems, surveys, techniques: high angular resolution, techniques: image processing, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics

الوصف: We present a new matched-filter algorithm for direct detection of point sources in the immediate vicinity of bright stars. The stellar point-spread function (PSF) is first subtracted using a Karhunen-Loéve image processing (KLIP) algorithm with angular and spectral differential imaging (ADI and SDI). The KLIP-induced distortion of the astrophysical signal is included in the matched-filter template by computing a forward model of the PSF at every position in the image. To optimize the performance of the algorithm, we conduct extensive planet injection and recovery tests and tune the exoplanet spectra template and KLIP reduction aggressiveness to maximize the signal-to-noise ratio (S/N) of the recovered planets. We show that only two spectral templates are necessary to recover any young Jovian exoplanets with minimal S/N loss. We also developed a complete pipeline for the automated detection of point-source candidates, the calculation of receiver operating characteristics (ROC), contrast curves based on false positives, and completeness contours. We process in a uniform manner more than 330 data sets from the Gemini Planet Imager Exoplanet Survey and assess GPI typical sensitivity as a function of the star and the hypothetical companion spectral type. This work allows for the first time a comparison of different detection algorithms at a survey scale accounting for both planet completeness and false-positive rate. We show that the new forward model matched filter allows the detection of 50% fainter objects than a conventional cross-correlation technique with a Gaussian PSF template for the same false-positive rate.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/3wb2h29wTest

المؤلفون: Rameau, Julien, Follette, Katherine B, Pueyo, Laurent, Marois, Christian, Macintosh, Bruce, Millar-Blanchaer, Maxwell, Wang, Jason J, Vega, David, Doyon, René, Lafrenière, David, Nielsen, Eric L, Bailey, Vanessa, Chilcote, Jeffrey K, Close, Laird M, Esposito, Thomas M, Males, Jared R, Metchev, Stanimir, Morzinski, Katie M, Ruffio, Jean-Baptiste, Wolff, Schuyler G, Ammons, SM, Barman, Travis S, Bulger, Joanna, Cotten, Tara, De Rosa, Robert J, Duchene, Gaspard, Fitzgerald, Michael P, Goodsell, Stephen, Graham, James R, Greenbaum, Alexandra Z, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Kalas, Paul, Konopacky, Quinn, Larkin, James E, Maire, Jérôme, Marchis, Franck, Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Perrin, Marshall D, Poyneer, Lisa, Rajan, Abhijith, Rantakyrö, Fredrik T, Marley, Mark S, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Thomas, Sandrine, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane

المصدر: The Astronomical Journal. 153(6)

مصطلحات موضوعية: instrumentation: adaptive optics, planet-disk interactions, planetary systems, stars: individual, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics

الوصف: We present H band spectroscopic and Hμ photometric observations of HD 100546 obtained with the Gemini Planet Imager and the Magellan Visible AO camera. We detect H band emission at the location of the protoplanet HD 100546 b, but show that the choice of data processing parameters strongly affects the morphology of this source. It appears point-like in some aggressive reductions, but rejoins an extended disk structure in the majority of the others. Furthermore, we demonstrate that this emission appears stationary on a timescale of 4.6 years, inconsistent at the 2σ level with a Keplerian clockwise orbit at 59 au in the disk plane. The H band spectrum of the emission is inconsistent with any type of low effective temperature object or accreting protoplanetary disk. It strongly suggests a scattered-light origin, as this is consistent with the spectrum of the star and the spectra extracted at other locations in the disk. A non-detection at the 5σ level of HD 100546 b in differential Hμ imaging places an upper limit, assuming the protoplanet lies in a gap free of extinction, on the accretion luminosity of 1.7 ? 10-4 L o and for 1 R Jup. These limits are comparable to the accretion luminosity and accretion rate of T-Tauri stars or LkCa 15 b. Taken together, these lines of evidence suggest that the H band source at the location of HD 100546 b is not emitted by a planetary photosphere or an accreting circumplanetary disk but is a disk feature enhanced by the point-spread function subtraction process. This non-detection is consistent with the non-detection in the K band reported in an earlier study but does not exclude the possibility that HD 100546 b is deeply embedded.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/90p4z8n6Test

المؤلفون: Follette, Katherine B, Rameau, Julien, Dong, Ruobing, Pueyo, Laurent, Close, Laird M, Duchêne, Gaspard, Fung, Jeffrey, Leonard, Clare, Macintosh, Bruce, Males, Jared R, Marois, Christian, Millar-Blanchaer, Maxwell A, Morzinski, Katie M, Mullen, Wyatt, Perrin, Marshall, Spiro, Elijah, Wang, Jason, Ammons, S Mark, Bailey, Vanessa P, Barman, Travis, Bulger, Joanna, Chilcote, Jeffrey, Cotten, Tara, De Rosa, Robert J, Doyon, Rene, Fitzgerald, Michael P, Goodsell, Stephen J, Graham, James R, Greenbaum, Alexandra Z, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Kalas, Paul, Konopacky, Quinn, Larkin, James E, Maire, Jérôme, Marchis, Franck, Metchev, Stanimir, Nielsen, Eric L, Oppenheimer, Rebecca, Palmer, David, Patience, Jennifer, Poyneer, Lisa, Rajan, Abhijith, Rantakyrö, Fredrik T, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Thomas, Sandrine, Vega, David, Wallace, J Kent, Ward-Duong, Kimberly, Wiktorowicz, Sloane, Wolff, Schuyler

المصدر: The Astronomical Journal. 153(6)

مصطلحات موضوعية: instrumentation: adaptive optics, planet-disk interaction, protoplanetary disk, stars: individual, astro-ph.EP, Astronomical and Space Sciences, Astronomy & Astrophysics

الوصف: We present optical and near-infrared high-contrast images of the transitional disk HD 100546 taken with the Magellan Adaptive Optics system (MagAO) and the Gemini Planet Imager (GPI). GPI data include both polarized intensity and total intensity imagery, and MagAO data are taken in Simultaneous Differential Imaging mode at Hα. The new GPI H-band total intensity data represent a significant enhancement in sensitivity and field rotation compared to previous data sets and enable a detailed exploration of substructure in the disk. The data are processed with a variety of differential imaging techniques (polarized, angular, reference, and simultaneous differential imaging) in an attempt to identify the disk structures that are most consistent across wavelengths, processing techniques, and algorithmic parameters. The inner disk cavity at 15 au is clearly resolved in multiple data sets, as are a variety of spiral features. While the cavity and spiral structures are identified at levels significantly distinct from the neighboring regions of the disk under several algorithms and with a range of algorithmic parameters, emission at the location of HD 100546 "c" varies from point-like under aggressive algorithmic parameters to a smooth continuous structure with conservative parameters, and is consistent with disk emission. Features identified in the HD 100546 disk bear qualitative similarity to computational models of a moderately inclined two-armed spiral disk, where projection effects and wrapping of the spiral arms around the star result in a number of truncated spiral features in forward-modeled images.

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/0bd737z4Test

المؤلفون: Johnson-Groh, Mara, Marois, Christian, De Rosa, Robert J, Nielsen, Eric L, Rameau, Julien, Blunt, Sarah, Vargas, Jeffrey, Ammons, S Mark, Bailey, Vanessa P, Barman, Travis S, Bulger, Joanna, Chilcote, Jeffrey K, Cotten, Tara, Doyon, Rene, Duchene, Gaspard, Fitzgerald, Michael P, Follette, Kate B, Goodsell, Stephen, Graham, James R, Greenbaum, Alexandra Z, Hibon, Pascale, Hung, Li-Wei, Ingraham, Patrick, Kalas, Paul, Konopacky, Quinn M, Larkin, James E, Macintosh, Bruce, Maire, Jerome, Marchis, Franck, Marley, Mark S, Metchev, Stanimir, Millar-Blanchaer, Maxwell A, Oppenheimer, Rebecca, Palmer, David W, Patience, Jenny, Perrin, Marshall, Poyneer, Lisa A, Pueyo, Laurent, Rajan, Abhijith, Rantakyroe, Fredrik T, Savransky, Dmitry, Schneider, Adam C, Sivaramakrishnan, Anand, Song, Inseok, Soummer, Remi, Thomas, Sandrine, Vega, David, Wallace, J Kent, Wang, Jason J, Ward-Duong, Kimberly, Wiktorowicz, Sloane J, Wolff, Schuyler G

المصدر: ASTRONOMICAL JOURNAL. 153(4)

مصطلحات موضوعية: planetary systems, stars: individual, Astronomy & Astrophysics, Astronomical and Space Sciences

وصف الملف: application/pdf

الوصول الحر: https://escholarship.org/uc/item/4jk7b8xgTest